ESPRESSO: The VLT planet hunter

Overview

ESPRESSO is the ESO/VLT high-resolution spectrograph to measure precise radial velocities on a long timespan with the main scientific aim of detecting and characterising Earth twins in the habitable zone of solar-like stars.

ESPRESSO is a highly-stabilized fibre-fed échelle spectrograph that can be fed with light from either a single or the four Unit Telescopes simultaneously. The instrument is installed at the incoherent combined Coudé focus (ICCF) of the VLT. The light from an astronomical source is redirected from the telescopes to the detectors through three components of the ICCF facility: the Coudé trains, the front ends, and the spectrograph itself. The Coudé Trains (CT) bring the light from each telescope to the Combined Coudé Lab (CCL) through 13 optical elements, including mirrors, lenses, and prisms. The four Front Ends (one for each UT) receive the light from the CTs and feed the spectrograph entrance fibres. The Fibre Link transports the light from the Front Ends to the vacuum vessel. The latter is thermally stabilized at the mK level. The light is then going through the optical components of the spectrograph and splitted up into a red and a blue spectrum which are recorded on the corresponding science detectors.

The spectrograph is fed by two fibres, one for the target and the other for simultaneous calibration (either sky or simultaneous reference: Laser Frequency Comb, Fabry-Pérot, or Thorium-Argon lamp). The light from the two fibres is recorded onto a blue (380-525nm) and a red (525-788nm) CCD mosaic. ESPRESSO can operate in three different instrument configurations: High Resolution 1-UT (HR), Ultra High-Resolution 1-UT (UHR) and Medium Resolution 4-UT (MR). The main characteristics of each of these modes are summarised below (for more detailed information about the characteristics of the instrument, see the Instrument Description).

 

HR (1-UT) UHR (1-UT)

MR (4-UT)

[not offered in P102]

Wavelength range 380–788 nm  380–788 nm  380–788 nm 
Resolving power (median) 140,000 190,000 70,000
Aperture on sky 1''.0 0''.5 4x1''.0
Global efficiency @ 550nm 9% 4% 9%
RV precision (requirement)
< 10 cm/s < 5 m/s < 5 m/s
Limiting V-band magnitude* ~17 ~16 ~20
Binning 1x1, 2x1 1x1 4x2, 8x4
Spectral sampling (average) 4.5 px 2.5 px 5.5 px (binned x2)
Spatial sampling per slice 9.0 (4.5) px 5.0 px 5.5 px (binned x4)
Number of slices 2 2 2

* based on approximate S/N per pixel <10 in one hour.

Project details

Principal Investigators

  • PI: Francesco Pepe (Observatoire de Genève)
  • Co-PI: Stefano Cristiani (INAF - Trieste)
  • Co-PI: Rafael Rebolo (IAC)
  • Co-PI: Nuno Santos (CAUP, U. do Porto)
Project responsibles
  • Project Manager: Denis Mégevand (Observatoire de Genève)
  • Project Scientist: Paolo Molaro (INAF - Trieste)
Builders
  • Observatoire de Genève and University of Bern (Switzerland)
  • INAF - Trieste and Brera (Italy)
  • Instituto de Astrofísica de Canarias (Spain)
  • Universidade do Porto, and Lisboa (Portugal)
  • European Southern Observatory (ESO)
Relevant references
Instrument
science team
E. Emsellem (ESO, Chair), C. Aerts (Instituut voor Sterrenkunde, Leuven, Belgium), M. Haehnelt (Institute of Astronomy, Cambridge, UK), A. Hatzes (Thringer Landessternwarte, Tautenburg, Germany), V. Hill (Observatoire de la Côte d'Azur, France), G. Tinetti (University College London, London, UK)
ESO responsibles

 

Project useful links